Typical accretion process for simulation G101Dn5In4n3 where the outflows are suppressed. Panel (a) shows the density distribution (color scale), poloidal velocity field (black arrows), and magnetic field lines (solid white lines). The scale of the poloidal velocity is shown at the top right of the panel, and the magnetic field lines are depicted by the contours of the poloidal magnetic flux at several specific levels. Panel (b) illustrates the specific angular momentum, j_z = Rv_ϕ, normalized by the reference value ﹩{j}_{z0}=\sqrt{G{M}_{{\rm{pl}}}{r}_{{\rm{pl}}}}﹩ (color scale and contours). Panel (c) presents τ_a,mag (color scale) superposed with streamlines of −RB_ϕB_pol, applying a symmetrical logarithmic color scale with the range from −10⁻³ to 10⁻³ shown in linear scale while the other parts in logarithmic scale. In both panels (b) and (c), black dashed lines indicate the contours of the critical density ﹩{\rho }_{{\rm{crit}}}=100\,{\rho }_{{\rm{\inf }}}﹩, aiding in the identification of the disk profile. Violet dashed lines in panels (a)–(c) mark the boundaries where the azimuthal velocity reaches 80% of the Keplerian velocity (where ﹩{v}_{\phi }=0.8\sqrt{G{M}_{{\rm{pl}}}/r}﹩). For reference, the escape velocity and the Keplerian timescale at the planetary radius (r_pl = 0.0027 r_H) are v_esc = 27v_KH and ﹩{{\rm{\Omega }}}_{{\rm{K}}}^{-1}=1.4\times 1{0}^{-4}\,{{\rm{\Omega }}}_{{\rm{KH}}}^{-1}﹩, respectively.